SuzakuSuzaku observations of AGN and synergy with GLAST observations of AGN and synergy with GLAST

Jun Jun KataokaKataoka (Tokyo Tech) (Tokyo Tech) in collaboration with in collaboration with T.TakahashiT.Takahashi , ,G.MadejskiG.Madejski, , T.KamaeT.Kamae,,

S.WatanabeS.Watanabe, , M.UshioM.Ushio, , T.KohmuraT.Kohmura and and SuzakuSuzaku team team

PKS1510-089 (Suzaku)

OutlineOutline About Suzaku

Highlights from Suzaku

New GeV source

- TeV blazars

- Payloads & advantages

- ToO by GLAST trg

- Nearby FR-I/II

- Mission status

- GeV blazars

Summary

- BLRG

SuzakuSuzaku –– overview overview 5th Japanese X-ray astronomy satellite to study

- structure formation of the universe- structure formation of the universe

- environment very close to black holes- environment very close to black holes

by using- high-resolution X-ray spectroscopy- high-resolution X-ray spectroscopy

- wide-band X-ray spectroscopy- wide-band X-ray spectroscopy

Highly complementary to Chandra & XMM

Successfully launched on July 10, 2005 with JAXA’s M-V rocket

SuzakuSuzaku in the final ground test in the final ground test

> 300 sources have been observed by the end of Jan 2007

Science payloads of Science payloads of SuzakuSuzaku

X-ray spectrometer (XRS: 0.3-10 keV)

Hard X-ray detedtor (HXD: 10-600 keV)

X-ray imaging spectrometer (XIS:0.3-10 keV)

Advantages of Advantages of SuzakuSuzaku High S/N ratio between 0.3 and ~ 300 keV.

- ~1000 cm- ~1000 cm2 2 effective area for the XIS effective area for the XIS ((comparable to XMM at >5keVcomparable to XMM at >5keV))

- Extremely low background for both the XIS and HXD- Extremely low background for both the XIS and HXD

excellent spectral resolution especially below 1 keV.

Suzaku XISChandra ACIS

Spectrum of SNR E0102.2-729

Suzaku HXD

Background normalized by effective area

RXTE PCA

Why Why BlazarsBlazars with with SuzakuSuzaku??X-ray GeV γ TeV γoptical

ERCSSC

LE HELE peak(synchrotron)

HE peak(Inv. Comp)

θ

line of sight

jet axis

Jet is pointing close to our line of sight (θ ∼ a few deg).

Two distinct peak structures in the SED

-- brightness & rapid variability caused by relativistic beaming. brightness & rapid variability caused by relativistic beaming.

- Sync + inv. - Sync + inv. CopmtonCopmton, but wide variety (, but wide variety (blazarblazar sequence sequence).).

- Need - Need wide coveragewide coverage ; ; hard-X-ray properties are still poorly known!hard-X-ray properties are still poorly known!

“GeV” blazars

“TeV” blazars

SuzakuSuzaku view of Mrk421 (spectra) view of Mrk421 (spectra)

Mrk 421 was observed in Apr 2006 for a 40 ksec by Suzaku.

F2-10 keV ~ 18mCrab

Takahashi ++ 07Takahashi ++ 07

X-ray spectrum gradually curves toward high energies: - Γ1 ~ 1.9 (E<3 keV), Γ2 ~ 2.2 (3<E<18 keV), Γ3 ~ 3.0 (E>18 keV)

Suzaku 2006

from from ““peakpeak”” to to ““real endreal end”” of the Sync emission ! of the Sync emission !

- very bright phase, 1/3 of historical flare in 2001-02 (e.g., Cui 2004).

Sorry, preliminary- this figure is published very soon.

SuzakuSuzaku view of Mrk421 (variability) view of Mrk421 (variability)

Clear detection of “intra-day variability” at >10 keV ! - note excellent S/N, even above 10 - note excellent S/N, even above 10 keVkeV –– error bars are error bars are ““invisibleinvisible”…”…

Variability correlation, spectral evolution on Variability correlation, spectral evolution on hour-scale hour-scale possible with possible with GLASTGLAST, , VERITASVERITAS and and H.E.S.S ++.H.E.S.S ++.

GaidosGaidos++ 96++ 96

1 hr

Whipple(TeV)

Sorry, preliminary- this figure is published very soon.

SuzakuSuzaku view of PKS2155-304 (spectra) view of PKS2155-304 (spectra)

PKS2155 was observed for 65 ksec as a calibration target in 2005. - simultaneous with H.E.S.S: data processing by S.Wagner++

Unfortunately, it was in a historically low state (1/10 of flare state…), but we could determine the energy spectrum up to 50 keV. - a single steep PL of Γ ~ 2.6 well fit the data.

F2-10 keV = 1.4 mCrab

KohmuraKohmura++ 07++ 07

Suzaku 2006

SuzakuSuzaku view of PKS2155-304 (variability) view of PKS2155-304 (variability)

Rapid, large amplitude flare on ~hr scale.

A curious flare – the spectrum get “steeper” when brighter.

0 10.5 1.5Time [day]

0.5 1 2 5 10Energy [keV]

0.3-1 keV

3-10 keV

hardnesshardness

- smaller variability at higher energy - smaller variability at higher energy –– completely completely opposite opposite trend. trend. - a new challenge to shock acceleration theory ? - a new challenge to shock acceleration theory ?

flare

am

plitu

de

coun

ts s

-1

3hr

PKS2155 (Suzaku)

SuzakuSuzaku view of PKS1510-089 (spectra) view of PKS1510-089 (spectra)

soft excess!

Intensive monitoring over 3 days (120 ksec chunk of data).

F2-10 keV = 0.5 mCrab

Hard spectrum (Γ = 1.2) up to 60 keV with a soft excess.

-- unordinary flat electron population; unordinary flat electron population; N(N(γγ) ) ∝ ∝ γ γ -1.4-1.4

-- soft excess is fitted either by soft excess is fitted either by disk-BB (~0.2keV)disk-BB (~0.2keV) or steep PL or steep PL (Γ(Γ ~ 3.0 ~ 3.0).).

KataokaKataoka & & MadejskiMadejski ++ 07 ++ 07

PKS1510-089(Suzaku)

SuzakuSuzaku view of PKS1510-089 (variability) view of PKS1510-089 (variability)

Swift UVOT

Suzaku

Variability pattern is different only below 1 keV !

MW analysis are still on going - thanks for all collaborators!

0.4-1 keV

3-10 keV

12-40 keV

0 1 2 3Time [day]

Swift UVOT/XRT … P.Roming, optical … G.Tosti ++. RATAN 600 … Y.Kovalev, ATCA … P.EdwardsTheory … M.Sikora, L.Stawarz, R.Moderski ++

-- again, suggesting completely different origin for the soft excess! again, suggesting completely different origin for the soft excess!

KataokaKataoka ++ 07b ++ 07b

More close look at More close look at ““soft excesssoft excess””

blue bump

BC bump

Cold pair plasma should upscatter UV photons (“blue bump”) via the Bulk-Comptonization (BC) to EBC ~ ΓBLK

2Ediff ~ 1 keV.

A clue to “matter content of jet” : LBC,46 ∝ (ne/np) Ljet, 46

soft excess(BC or Sync tail ??)

0.5 1 5 10 50Energy [keV]

10-4

10-3

10-2

ν F

ν [

keV

/cm

2/s

]

-- but can we safely reject contaminationbut can we safely reject contamination from the Sync tail ? from the Sync tail ? optical/UV data importantoptical/UV data important

-- X-ray precursor before the X-ray precursor before the γγ-ray (-ray (GeVGeV) flare ?) flare ? ((ModerskiModerski ++ 04, Celloti++07) ++ 04, Celloti++07) GLAST strongly awaited !GLAST strongly awaited !

SikoraSikora++ 94++ 94PKS1510-089(Suzaku)

SuzakuSuzaku ToOToO by GLAST trigger by GLAST trigger

0 5 10 15 20 25 Time [day]

SuzakuToO level

We are proposing ToO monitoring of GeV flare with Suzaku (PI:JK) as well as persistent obs. (PI: GM).

F > 2x10-6 ph/cm2/s 200 ksec for 1 of 5 src

If accepted, data will be open to all GLAST team without delay.

Simulation!

Suzaku 3C279

New New GeVGeV Sources? : Sources? : mismis-aligned -aligned blazarsblazars

Chandra /VLA(Hardcastle++ 03)

F2-10 keV = 9mCrab

Not many, but nearby FR-I/ II galaxies can be detected as “mis-aligned” blazars. (e.g., Cen A, M87 etc…)

“unification scheme” of blazars & RG.

low power FR I TeV blazars

high power FR II GeV blazars

GLAST 1 yr

CenA

MarkowitzMarkowitz ++07 ++07 reconstructed from reconstructed from ChiabergeChiaberge++ 00++ 00

New New GeVGeV Sources? : Broad Line Radio Sources? : Broad Line Radio GlaxiesGlaxies (1) (1)

3C1203C120 (high state)(high state) (low state)(low state)

Variable PLVariable PL

1 5 10 50 1 5 10 50Energy [keV] Energy [keV]

Chandra

Broad emission lines, but also has extended jet emission (“composite”of Sy + RG.)

Suzaku discovered that the variability is mainly caused by a steep PL of Γ ~ 2.7.

kpc-jet

3C120

KataokaKataoka ++07a ++07a

3C120: 40ksec x 4 observations in 2006.

New New GeVGeV Sources? : Broad Line Radio Sources? : Broad Line Radio GlaxiesGlaxies (2) (2)

Suzaku; high - low

GLAST 1yr

If variable component originates from the Sync emission of “hidden jet”, IC emission can be detectable with GLAST.

Similar conclusion was made by direct fitting the SED with a “composite” disk and jet model ((GrandiGrandi++ 07; P12.8 this meeting)++ 07; P12.8 this meeting)

Other GLASTOther GLAST candidates : candidates : 3C390.3, 3C382, 3C111, 3C445 ++3C390.3, 3C382, 3C111, 3C445 ++

3C273

3C120

SummarySummary

I have reviewed recent observational highlights from Suzaku and synergy with GLAST.

Deep & wide MW monitoring will provide “new” blazar physics even for well-known sources;

TeV blazars … acceleration limit, hr-scale evolution…

GeV blazars … Bulk Compton, jet content… /ToO!

A number of non-blazar type AGN will be also detected for the first time in GeV band

nearby FR-I … “mis-aligned” blazars?

BLRG … evidence for hidden jet ? unification of RL & RQ AGN